Supercritical Accretion Flows around Black Holes: Two-dimensional, Radiation Pressure-dominated Disks with Photon Trapping

By K. Ohsuga, Masao Mori, T. Nakamoto, S. Mineshige. 2005

349 citations recorded by the source corpus.

The quasi-steady structure of supercritical accretion flows around a black hole is studied based on two-dimensional radiation-hydrodynamic (2D-RHD) simulations. The supercritical flow is composed of two parts: the disk region and the outflow regions above and below the disk. Within the disk region the circular motion and the patchy density structure are observed, which is caused by Kelvin-Helmholtz instability and probably by convection. The mass accretion rate decreases inward, roughly in proportion to the radius, and the remaining part of the disk material leaves the disk to form the outflow because of the strong radiation pressure force. We confirm that photon trapping plays an important role within the disk. Thus, matter can fall onto the black hole at a rate exceeding the Eddington rate. The emission is highly anisotropic and moderately collimated so that the apparent luminosity can exceed the Eddington luminosity by a factor of a few in the face-on view. The mass accretion rate onto the black hole increases with the absorption opacity (metallicity) of the accreting matter. This implies that the black hole tends to grow faster in metal-rich regions, such as in starburst galaxies or star-forming regions.

Subfields: Astronomy and Astrophysics, Immunology, Mechanical Engineering

View Paper: https://www.semanticscholar.org/paper/a76b69ff59fab288a773407daf1fe38ac03efc22

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Citations in the corpus

Super-Eddington Accretion Disks around Supermassive Black Holes (2017, methodology): “…model (Abramowicz et al. 1980) is often used to describe accretion disks in this regime and there have been a number of numerical simulations to study the properties of superEddington accretion disks recently (Ohsuga et al. 2005; Jiang et al. 2014a; McKinney et al. 2014; Sa̧dowski et al. 2014).”
Swift J1644+57 gone MAD: the case for dynamically-important magnetic flux threading the black hole in a jetted tidal disruption event (2013, background): “When the accretion rate is superEddington at early times, the disk may be prone to outflows driven by radiation pressure (e.g. Ohsuga et al. 2005; Strubbe & Quataert 2009), in which case the accretion rate reaching the BH is less than Ṁfb.”
A bright year for tidal disruptions (2015, methodology): “…Events 5 η ≈ 0.05 for a non-rotating BH was found by radiation (magneto)hydrodynamical simulations of highly super-Eddington disk accretion (e.g. Jiang et al. 2014; see also Ohsuga et al. 2005; Sadowski & Narayan 2015; Jiao et al. 2015), when both radiative and kinetic luminosity are considered.”
Neutrino-dominated accretion flows as the central engine of gamma-ray bursts (2017, background): “(I) Neutrino trapping radius rtrap Photon trapping may occur in the supercritical accretion disk if the time of photon diffusion from the equatorial plane of the disk to the surface is longer than the accretion timescale (e.g., Katz 1977; Begelman 1978; Ohsuga et al. 2002, 2005).”
Supercritically accreting stellar mass black holes as ultraluminous X-ray sources (2006, methodology): “Together these effects result in the 10–30- fold excess overLEdd at high accretion rates (see also Ohsuga et al. 2005; Begelman et al. 2006; Fabrika et al. 2006).”
Finite, Intense Accretion Bursts from Tidal Disruption of Stars on Bound Orbits (2012, background): “Although the fate of the circularized debris is unclear because of much shorter simulation time than the viscous timescale, the super-Eddington accretion flow will likely drive a powerful outflow (Ohsuga et al. 2005) as it becomes radiation-pressure dominated.”
Hot Accretion Flows Around Black Holes (2014, background): “optically thick advection-dominated accretion flow (Katz 1977, Begelman 1979, Begelman & Meier 1982, Abramowicz et al. 1988, Chen & Taam 1993, Ohsuga et al. 2005).”
Optical Flares from the Tidal Disruption of Stars by Massive Black Holes (2009, background): “The gas is likely to form an advective accretion disk accompanied by powerful outflows (e.g., Ohsuga et al. 2005), although the relative importance of accretion and outflows in this phase is somewhat uncertain (see §6).”
Global Radiation-Magnetohydrodynamic Simulations of Black-Hole Accretion Flow and Outflow: Unified Model of Three States (2009, methodology): “We find that the radiation energy density (Erad) is very large in the disk region, and the steep profile of Erad enhances the radiation force (radiative flux) (Ohsuga et al. 2005).”
GLOBAL STRUCTURE OF THREE DISTINCT ACCRETION FLOWS AND OUTFLOWS AROUND BLACK HOLES FROM TWO-DIMENSIONAL RADIATION-MAGNETOHYDRODYNAMIC SIMULATIONS (2011, background): “In the conventional disk models and in the radiation hydrodynamic simulations, in contrast, the phenomenological viscosity (α-viscosity) induces the angular-momentum transfer as well as the energy dissipation (Eggum et al. 1988; Okuda & Fujita 2000; Ohsuga et al. 2005b; Ohsuga 2006).”
Ultraluminous X-ray sources in the Chandra and XMM-Newton era (2011, background): “…2009; Takeuchi et al. 2010; Mineshige & Ohsuga 2011) supported and advanced earlier analytical results (slim disk models; Abramowicz et al. 1988; Watarai et al. 2001; Ebisawa et al. 2003; Heinzeller & Duschl 2007), and the radiation-hydrodynamical simulations of, among others, Ohsuga et al. (2005).”
Three-dimensional general relativistic radiation magnetohydrodynamical simulation of super-Eddington accretion, using a new code HARMRAD with M1 closure (2013, methodology): “…code and flux-limited diffusion, super-Eddington accretion flows have been simulated and their spectra computed (Ohsuga et al. 2003; Ohsuga et al. 2005; Ohsuga 2006; Ohsuga et al. 2009; Ohsuga & Mineshige 2011; Kawashima et al. 2012; Mineshige et al. 2012; Takeuchi et al. 2013;…”
A GLOBAL THREE-DIMENSIONAL RADIATION MAGNETO-HYDRODYNAMIC SIMULATION OF SUPER-EDDINGTON ACCRETION DISKS (2014, methodology): “Comparison with Previous Simulations Super-Eddington accretion disks for non-spinning black holes have been studied extensively with 2D axisymmetric radiation hydro or MHD simulations (Ohsuga et al. 2005, 2009; Ohsuga & Mineshige 2011, 2013; Sa̧dowski et al. 2014).”
A Unified Model for Tidal Disruption Events (2018, background): “Recently the development of novel radiation magnetohydrodynamics (MHD) codes, some of which also performed under full general relativity (GR), have helped us understand more about such accretion flow (e.g., Ohsuga et al. 2005; Jiang et al. 2014; McKinney et al. 2014; Sa̧dowski et al. 2015).”
Hyper-Eddington accretion flows on to massive black holes (2015, background): “…and jets from the inner accretion disk in the vertical direction could potentially break the hyper-Eddington accretion solution (e.g. Begelman 2002; Ohsuga et al. 2005, 2009; Dotan & Shaviv 2011; Li, Ostriker & Sunyaev 2013; Jiang, Stone & Davis 2014; McKinney et al. 2014; Sa̧dowski et al. 2015;…”
Rates of stellar tidal disruption as probes of the supermassive black hole mass function (2014, background): “Such disks are believed to drive mildly relativistic outflows, a process that has been modeled analytically (Blandford & Begelman 1999; Strubbe & Quataert 2009) and numerically (Ohsuga et al. 2005; Sadowski et al. 2014).”
What drives the growth of black holes (2011, background): “Hydrodynamical simulations of BHs accreting at superEddington rates indeed predict the presence of a radiatively driven high-column density wind (Ohsuga et al., 2005; Ohsuga, 2007), providing indirect support for this model.”